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1. Constraining the Properties of the Multicomponent Local Interstellar Medium: MHD-kinetic Modeling Validated by Voyager and New Horizons Data

   https://doi.org/10.3847/2041-8213/ad7e1c  

   Fraternale, Federico; Pogorelov, Nikolai V; Bera, Ratan K (October 2024, The Astrophysical Journal Letters)

   Abstract We introduce the first solar-cycle simulations from our 3D, global MHD-plasma/kinetic-neutrals model, where both hydrogen and helium atoms are treated kinetically, while electrons and helium ions are described as individual fluids. Using Voyager/PWS observations of electron density up to 160 au from the Sun for validation of several different global models, we conclude that the current estimates for the proton density in the local interstellar medium (LISM) need a revision. Our findings indicate that the commonly accepted value of 0.054 cm⁻³may need to be increased to values exceeding 0.07 cm⁻³. We also show how different assumptions regarding the proton velocity distribution function in the outer heliosheath may affect the global solution. A new feature revealed by our simulations is that the helium ion flow may be significantly compressed and heated in the heliotail at heliocentric distances exceeding ∼400 au. Additionally, we identify a Kelvin–Helmholtz instability at the boundary of the slow and fast solar wind in the inner heliosheath, which acts as a driver of turbulence in the heliotail. These results are crucial for inferring the properties of the LISM and of the global heliosphere structure. 

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2. The Long-lived Broadband Afterglow of Short Gamma-Ray Burst 231117A and the Growing Radio-detected Short Gamma-Ray Burst Population

   https://doi.org/10.3847/1538-4357/ada9e5  

   Schroeder, Genevieve; Fong, Wen-fai; Kilpatrick, Charles D; Rouco_Escorial, Alicia; Laskar, Tanmoy; Nugent, Anya E; Rastinejad, Jillian; Alexander, Kate D; Berger, Edo; Brink, Thomas G; et al (March 2025, The Astrophysical Journal)

   Abstract We present multiwavelength observations of the Swift shortγ-ray burst GRB 231117A, localized to an underlying galaxy at redshiftz= 0.257 at a small projected offset (∼2 kpc). We uncover long-lived X-ray Chandra X-ray Observatory and radio/millimeter (VLA, MeerKAT, and ALMA) afterglow emission, detected to ∼37 days and ∼20 days (rest frame), respectively. We measure a wide jet (∼10 $\stackrel{\text{°}}{.}$4) and relatively high circumburst density (∼0.07 cm⁻³) compared to the short GRB population. Our data cannot be easily fit with a standard forward shock model, but they are generally well fit with the incorporation of a refreshed forward shock and a reverse shock at <1 day. We incorporate GRB 231117A into a larger sample of 132 X-ray detected events, 71 of which were radio-observed (17 cm-band detections), for a systematic study of the distributions of redshifts, jet and afterglow properties, galactocentric offsets, and local environments of events with and without detected radio afterglows. Compared to the entire short GRB population, the majority of radio-detected GRBs are at relatively low redshifts (z < 0.6) and have high circumburst densities (>10⁻²cm⁻³), consistent with their smaller (<8 kpc) projected galactocentric offsets. We additionally find that 70% of short GRBs with opening angle measurements were radio-detected, indicating the importance of radio afterglows in jet measurements, especially in the cases of wide (>10°) jets where observational evidence of collimation may only be detectable at radio wavelengths. Owing to improved observing strategies and the emergence of sensitive radio facilities, the number of radio-detected short GRBs has quadrupled in the past decade. 

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3. A continuum of amorphous ices between low-density and high-density amorphous ice

   https://doi.org/10.1038/s42004-024-01117-2  

   Eltareb, Ali; Lopez, Gustavo E; Giovambattista, Nicolas (February 2024, Communications Chemistry)

   Abstract Amorphous ices are usually classified as belonging to low-density or high-density amorphous ice (LDA and HDA) with densitiesρ_LDA ≈ 0.94 g/cm³andρ_HDA ≈ 1.15−1.17 g/cm³. However, a recent experiment crushing hexagonal ice (ball-milling) produced amedium-density amorphous ice (MDA,ρ_MDA ≈ 1.06 g/cm³) adding complexity to our understanding of amorphous ice and the phase diagram of supercooled water. Motivated by the discovery of MDA, we perform computer simulations where amorphous ices are produced by isobaric cooling and isothermal compression/decompression. Our results show that, depending on the pressure employed, isobaric cooling can generate a continuum of amorphous ices with densities that expand in between those of LDA and HDA (briefly, intermediate amorphous ices, IA). In particular, the IA generated atP ≈ 125 MPa has a remarkably similar density and average structure as MDA, implying that MDA is not unique. Using the potential energy landscape formalism, we provide an intuitive qualitative understanding of the nature of LDA, HDA, and the IA generated at different pressures. In this view, LDA and HDA occupy specific and well-separated regions of the PEL; the IA prepared atP = 125 MPa is located in the intermediate region of the PEL that separates LDA and HDA. 

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4. First predicted cosmic ray spectra, primary-to-secondary ratios, and ionization rates from MHD galaxy formation simulations

   https://doi.org/10.1093/mnras/stac1791  

   Hopkins, Philip F.; Butsky, Iryna S.; Panopoulou, Georgia V.; Ji, Suoqing; Quataert, Eliot; Faucher-Giguère, Claude-André; Kereš, Dušan (July 2022, Monthly Notices of the Royal Astronomical Society)

   ABSTRACT We present the first simulations evolving resolved spectra of cosmic rays (CRs) from MeV–TeV energies (including electrons, positrons, (anti)protons, and heavier nuclei), in live kinetic-magnetohydrodynamics galaxy simulations with star formation and feedback. We utilize new numerical methods including terms often neglected in historical models, comparing Milky Way analogues with phenomenological scattering coefficients ν to Solar-neighbourhood [Local interstellar medium (LISM)] observations (spectra, B/C, e+/e−, $$\mathrm{\bar{p}}/\mathrm{p}$$, 10Be/9Be, ionization, and γ-rays). We show it is possible to reproduce observations with simple single-power-law injection and scattering coefficients (scaling with rigidity R), similar to previous (non-dynamical) calculations. We also find: (1) The circumgalactic medium in realistic galaxies necessarily imposes an $$\sim 10\,$$ kpc CR scattering halo, influencing the required ν(R). (2) Increasing the normalization of ν(R) re-normalizes CR secondary spectra but also changes primary spectral slopes, owing to source distribution and loss effects. (3) Diffusive/turbulent reacceleration is unimportant and generally sub-dominant to gyroresonant/streaming losses, which are sub-dominant to adiabatic/convective terms dominated by $$\sim 0.1-1\,$$ kpc turbulent/fountain motions. (4) CR spectra vary considerably across galaxies; certain features can arise from local structure rather than transport physics. (5) Systematic variation in CR ionization rates between LISM and molecular clouds (or Galactic position) arises naturally without invoking alternative sources. (6) Abundances of CNO nuclei require most CR acceleration occurs around when reverse shocks form in SNe, not in OB wind bubbles or later Sedov–Taylor stages of SNe remnants. 

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5. The 107 GHz Methanol Transition Is a Dasar in G0.253+0.016

   https://doi.org/10.3847/1538-4357/acf0c1  

   Bulatek, Alyssa; Ginsburg, Adam; Darling, Jeremy; Henkel, Christian; Menten, Karl M. (October 2023, The Astrophysical Journal)

   Abstract We present observations of population anti-inversion in the 3₁− 4₀A⁺transition of CH₃OH (methanol) at 107.013831 GHz toward the Galactic center cloud G0.253+0.016 (“The Brick”). Anti-inversion of molecular level populations can result in absorption lines against the cosmic microwave background (CMB) in a phenomenon known as a “dasar.” We model the physical conditions under which the 107 GHz methanol transition dases and determine that dasing occurs at densities below 10⁶cm⁻³and column densities between 10¹³and 10¹⁶cm⁻². We also find that for this transition, dasing does not strongly depend on the gas kinetic temperature. We evaluate the potential of this tool for future deep galaxy surveys. We note that other works have already reported absorption in this transition (e.g., in NGC 253), but we provide the first definitive evidence that it is absorption against the CMB rather than against undetected continuum sources. 

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